Yadav, N.; Cameron, R. H.; Solanki, S. K.: Simulations Show that Vortex Flows Could Heat the Chromosphere in Solar Plage. Astrophysical Journal, Letters 894 (2), L17 (2020)
Cameron, R. H.; Jiang, J.: The relationship between flux emergence and subsurface toroidal magnetic flux. Astronomy and Astrophysics; EDP Sciences, Les Ulis Cedex A France 631, A27 (2019)
Cameron, R. H.; Schüssler, M.: Solar activity: periodicities beyond 11 years are consistent with random forcing. Astronomy and Astrophysics 625, A28 (2019)
Nielsen, M. B.; Gizon, L.; Cameron, R. H.; Miesch, M.: Starspot rotation rates versus activity cycle phase: Butterfly diagrams of Kepler stars are unlike that of the Sun. Astronomy and Astrophysics 622, A85 (2019)
Boro Saikia, S.; Marvin, C. J.; Jeffers, S. V.; Reiners, A.; Cameron, R. H.; Marsden, S. C.; Petit, P.; Warnecke, J.; Yadav, A. P.: Chromospheric activity catalogue of 4454 cool stars: Questioning the active branch of stellar activity cycles. Astronomy and Astrophysics 616, A108 (2018)
Jafarzadeh, S.; Solanki, S. K.; Stangalini, M.; Steiner, O.; Cameron, R. H.; Danilovic, S.: High-frequency Oscillations in Small Magnetic Elements Observed with SUNRISE/SuFI. Astrophysical Journal, Suppl. Ser. 229 (1), 10 (2017)
Martin-Belda, D.; Cameron, R.: Inflows towards active regions and the modulation of the solar cycle: A parameter study. Astronomy and Astrophysics 597, A21 (2017)
First Light for Sunrise III: the first tests with real sunlight were successful. The balloon-borne solar observatory should be ready for launch at the end of May.
First icy cold, then midnight sun: at the Arctic Circle, the team will prepare the next flight of the balloon-borne solar observatory - and hopes for solar fireworks.
Astronomical teamwork: By combining data from Solar Orbiter and SDO, a group of researchers has unambiguously determined the magnetic field at the solar surface.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.